4U 1954+319

Light curves
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There are fake flares prominent in the soft (2-4 keV) band in every 70 days.
4U1954+319 was periodically contaminated by Cyg X-1.
The contamination is by the "tail" of the PSF on the image,
and the scan direction changes by the orbital presession period of
ISS (70 days). The contamination is stronger in the soft band
where the PSF is bigger, when MAXI cameras are operated with the reduced
high voltage (1550V) and when Cyg X-1 is in the soft-state.

The data is updated in every day.
The data was processed with version 7L, where both 1650V and 1550V data
are used.
Evaluation of the shadow of solar paddles are improved. This decreased the
number of dropping data points.
A-system camera 0 (gas leaking camera) is also used until 57900 MJD.
There, the flux has a large uncertainty (a few tens of % in 2-4 keV).
Even in 4-10 keV, the data have larger uncertainty than those in
the other normal cameras.
After 57900 MJD, A-system Camera 0 is no-longer used in version 7L,
and the data have smaller error bars, although data gaps appears
for some sources.

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